The role of inner disk edges in shaping ultra-short-period planet systems around late M dwarfs

Open Access

Table 1

Summary of scenarios explored in this study.

Scenario	Prescription for r_in	Range of r_in [au]
FIX	Fixed inner edge at P_* = 1 d (near corotation).	Constant at 0.01
OUT[M]	Magnetospheric truncation with $B_{⋆} \propto R_{⋆}^{- 2}$ $Mathematical equation: $B_\star \propto R_\star^{-2}$$ (initial B₀ = 200 G, R₀ = 1.003 R_⊙); r_in = r_m(t) drifts outward with time.	0.020-0.036
IN[C]	r_in = r_cor(t) with P_*,ini = 5 d; r_in contracts → moves inward with stellar spin-up.	0.027-0.008

Notes. Rotation values correspond to the stellar period for which r_in ≈ r_cor at 1 Myr. The resulting range of the inner disk edge during the disk lifetime (up to ~ 10 Myr) is also listed.

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